Dense gas in low-metallicity galaxies
arXiv:1612.02196 · doi:10.1051/0004-6361/201629781
Abstract
Stars form out of the densest parts of molecular clouds. Far-IR emission can be used to estimate the Star Formation Rate (SFR) and high dipole moment molecules, typically HCN, trace the dense gas. A strong correlation exists between HCN and Far-IR emission, with the ratio being nearly constant, over a large range of physical scales. A few recent observations have found HCN to be weak with respect to the Far-IR and CO in subsolar metallicity (low-Z) objects. We present observations of the Local Group galaxies M33, IC10, and NGC6822 with the IRAM 30meter and NRO 45m telescopes, greatly improving the sample of low-Z galaxies observed. HCN, HCO, CS, CH, and HNC have been detected. Compared to solar metallicity galaxies, the Nitrogen-bearing species are weak (HCN, HNC) or not detected (CN, HNCO, NH) relative to Far-IR or CO emission. HCO and CH emission is normal with respect to CO and Far-IR. While CO is the usual factor 10 weaker than CO, CO emission was not detected down to very low levels. Including earlier data, we find that the HCN/HCO ratio varies with metallicity (O/H) and attribute this to the sharply decreasing Nitrogen abundance. The dense gas fraction, traced by the HCN/CO and HCO/CO ratios, follows the SFR but in the low-Z objects the HCO is much easier to measure. Combined with larger and smaller scale measurements, the HCO line appears to be an excellent tracer of dense gas and varies linearly with the SFR for both low and high metallicities.
arXiv comment9 pages, 13 figures, A&A in press
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